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超声速磁流体加速实验及一维模型分析 总被引:2,自引:1,他引:1
为了获得负载系数、电导率等参数变化对超声速磁流体加速效果的影响规律,利用激波风洞,采用氩气与碳酸钾作为工质,电容提供电能的方式,在磁感应强度为0.5T的条件下,进行了不同电容充电电压下的超声速磁流体加速实验研究,并对一维定常理想分段法拉第型磁流体加速模型进行了分析.通过实验获得了不同电容充电电压下#10电极间的电压、电流、负载系数、电导率及#20电极开路电压等数据,在300, 400V电容充电电压下,气流速度分别增加11.4%和24.0%,在500V电容充电电压下气流速度减小11.1%.实验及模型分析得出不同的负载系数会使超声速磁流体处于加速或减速的不同状态,而电导率会影响注入总能量的大小,使磁流体流动的速度梯度大小发生改变. 相似文献
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为了开展磁流体(MHD)流动控制原理研究,建立了磁流体技术试验系统,采用电容耦合射频-直流组合放电对Ma=3.5气流进行电离,在磁场作用下产生顺/逆气流方向的洛伦兹力控制流场,采用试验段静压变化来监测磁流体流动控制效果,通过一维模型计算磁流体流动控制过程中流场变化情况,分析磁流体流动控制效果;通过添加电磁源项的Navier-Stokes方程耦合电势泊松方程建立了二维磁流体动力模型,对磁流体流动控制进行数值模拟研究。主要结论如下:在磁场约束下,电容耦合射频-直流组合放电能够在Ma=3.5流场中产生大体积均匀电流,电导率约0.015S/m;在焦耳热和洛伦兹力作用下,磁流体加速时静压升高了130Pa,减速时静压升高了200Pa;磁流体流动控制过程中,仅有不足10%的能量在磁流体通道内发生了作用;数值模拟结果显示,在试验条件下,加速时静压升高了128Pa,减速时静压升高了208Pa,与试验结果基本吻合。 相似文献
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准一维可压缩瞬变管流的有限体积模型(Ⅰ)流场的有限体积模型 总被引:1,自引:4,他引:1
针对现有流体系统一维动力学模型缺乏统一的理论推导过程和能够涵盖众多模型的基本方程组的现象,从适用于连续介质控制体的欧拉型积分形式的流动守恒方程出发,经过合理模化推导得到了可压缩变截面管流准一维瞬变流动积分形式和微分形式的守恒方程.通过保留能量方程中的变体积项考虑了由于控制体体积的改变所输出的膨胀功.通过对守恒方程在空间交错网格上的有限体积离散建立了一种计算准一维可压缩变截面管流瞬变流场的有限体积模型,该模型可考虑变体积、变物性、轴向热传导、重力场影响,一方面,在深化和阐明了有限元状态变量模型体系的理论基础的同时,拓宽了其对瞬变流动的适用范围,另一方面,结合阀芯节流模型,从此模型出发可推导出管路系统常见元件的流场模型. 相似文献
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为了获得高超声速低温来流条件下基于电子束电离的磁流体发电机性能,采用三维低磁雷诺数磁流体动力学五方程模型和简化的电子束电离模型,对等截面分段法拉第型磁流体发电机内的流动进行数值模拟,研究了电离能量花费、磁场强度对发电通道性能的影响,得出了不同电离花费下电离所形成的电子数密度和电导率.研究结果表明,电子束电离低温来流能够产生足够的电导率,当负载系数保持为0.5时,电效率基本保持在0.5 ~0.6之间,电效率大小受磁场强度影响不大,电离能量花费Pion(MW/m3)为0.06,0.6,6,30,300时的电导率σ(S/m)分别为0.28,0.9,3,7,27.当电离能量花费为30MW/m3,能量提取率达到26%,电效率为66%,发电机性能接近最佳,对应的磁场强度为10T. 相似文献
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研究了航天器推进系统管路充填过程动态模型与计算方法。以一维管道瞬变流理论为基础 ,采用瞬变管流湍流频率相关摩擦损失模型计算管壁摩擦流阻 ,构造了管路分支流阻计算模型 ,考虑了液流撞壁后的蒸汽泡团释出与崩溃现象。数值计算采用特征线方法 ,仿真结果表明计算模型较好地描述了充填过程中的水击和管流振荡现象 相似文献
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NND格式在多维理想磁流体方程组中的应用 总被引:3,自引:0,他引:3
采用修正的四步Runge-Kutta方法求解三维一般曲线坐标系下的理想磁流体方程组,为克服数值振荡,加特征型NND格式进行后处理.特征型NND格式推广到求解三维磁流体(MHD)问题需要知道雅可比通量的左右特征矩阵,在具体计算时需要克服矩阵的奇性.本文用三维程序采用推广的特征NND格式计算了一维MHD激波管和二维(MHD)喷管流动,计算结果表明,特征NND格式保持了TVD格式高精度的优点,又具有计算简单的特点,在包括强弱间断等复杂波系的定常和非定常MHD流场数值模拟中是成功的. 相似文献
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磁流体能量旁路超燃冲压发动机的混合 和燃烧性能数值研究 总被引:2,自引:0,他引:2
为了研究磁流体能量旁路超燃冲压发动机(AJAX)的混合燃烧性能,采用三维数值方法,分别对磁流体发电器作用区和化学反应区进行模拟.在其他条件不变的情况下,改变磁场强度和载荷因子从而改变燃烧室的入口条件,得到不同磁流体条件下的混合效率和燃烧效率.计算结果显示:随着磁场强度的增加和载荷因子的减小,混合效率都提高了,最多提高了11.4%,在热离解不明显的燃烧室前半段,燃烧效率也都有所提高;在燃烧室后半段,不出现热离解时燃烧效率最多提高6.5%,此时磁流体装置的引入可使燃烧室长度缩短25%,可降低飞行器的几何尺寸,减轻飞行器质量;出现热离解时,燃烧效率会有所降低甚至低于无磁流体作用时的情况,因此应尽量避免磁场强度过大或载荷因子过小引起燃烧室入口静温过高造成热离解降低燃烧效率. 相似文献
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高温气体电导率是高超声速电磁流动控制数值模拟最重要的参数之一。针对电导率模拟准确性及其对高超声速磁流体控制影响的问题,考虑高超声速飞行器流场中高温气体热化学非平衡效应,采用三维低磁雷诺数磁流体动力学(MHD)数值模拟方法及程序,结合国内外常见电导率处理方法开展典型状态高超声速MHD控制数值模拟,分析电导率模拟对高超声速磁流体流场分布、气动力/热特性的影响。研究表明:磁控热流减缓效果与电导率呈非线性关系,电导率较大时将出现电导率的磁控热饱和现象,其产生的原因可能与化学反应趋向于平衡态存在一定关系;采用定电导率方法,会人为放大磁场洛仑兹力的磁阻力效果,使阻力系数的预测值偏大;不同电导率模型计算得到的电导率分布差异很大,甚至存在数量级的差别,显著影响了磁流体的控制效果,这与电导率模型的适用范围、参数选取原则存在很大关联;对于含多种离解、电离组分的高温气体流动来说,采用基于多电离组分迁移碰撞的电导率模型(本文模型M8),计算与试验一致性最好。 相似文献
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Three major cusp models are systematically compared with low-resolution (large-scale) and high-resolution (fine-scale) low-altitude observations. Those models are (a) global magnetohydrodynamics (MHD) models (including MHD+drift models), (b) turbulent/diffusive entry models, and (c) direct flowing entry models. Although low-resolution data are mostly consistent with MHD models, high-resolution data mostly contradicts them. The data instead supports the other models in which the cusp is considered as a local `extra' open region. This is a good lesson to us: past supportive `tests' of MHD cusp models might have essential flaws in the methodology, and high-resolution data is necessary even for large-scale modelings. 相似文献
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A Class of TVD Type Combined Numerical Scheme for MHD Equations With a Survey About Numerical Methods in Solar Wind Simulations 总被引:3,自引:0,他引:3
It has been believed that three-dimensional, numerical, magnetohydrodynamic (MHD) modelling must play a crucial role in a
seamless forecasting system. This system refers to space weather originating on the sun; propagation of disturbances through
the solar wind and interplanetary magnetic field (IMF), and thence, transmission into the magnetosphere, ionosphere, and thermosphere.
This role comes as no surprise to numerical modelers that participate in the numerical modelling of atmospheric environments
as well as the meteorological conditions at Earth. Space scientists have paid great attention to operational numerical space
weather prediction models. To this purpose practical progress has been made in the past years. Here first is reviewed the
progress of the numerical methods in solar wind modelling. Then, based on our discussion, a new numerical scheme of total
variation diminishing (TVD) type for magnetohydrodynamic equations in spherical coordinates is proposed by taking into account
convergence, stability and resolution. This new MHD model is established by solving the fluid equations of MHD system with
a modified Lax-Friedrichs scheme and the magnetic induction equations with MacCormack II scheme for the purpose of developing
a combined scheme of quick convergence as well as of TVD property. To verify the validation of the scheme, the propagation
of one-dimensional MHD fast and slow shock problem is discussed with the numerical results conforming to the existing results
obtained by the piece-wise parabolic method (PPM). Finally, some conclusions are made.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
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针对飞行马赫数大于设计马赫数的情况,采用二维磁流体动力学方程对磁控进气道进行了数值模拟研究。数值模拟结果表明磁流体装置的电磁作用可以使非设计马赫数下进气道激波满足SOL(shock on lip)条件,并使出口处的流动变得均匀。分析了磁流体作用位置、宽度和深度等关键控制参数对该类进气道性能的影响,计算结果表明,磁流体作用区域越靠近飞行器前缘,而且在纵向越深,则进气道出口处的流动越均匀,但流率会有所下降;若磁流体作用区域较宽,则需较小的磁场就能使非设计马赫数下进气道的激波结构满足SOL条件。 相似文献
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Leon Ofman 《Space Science Reviews》2005,120(1-2):67-94
Coronal holes have been identified as source regions of the fast solar wind, and MHD wave activity has been detected in coronal
holes by remote sensing, and in situ in fast solar wind streams. I review some of the most suggestive wave observations, and
discuss the theoretical aspects of MHD wave heating and solar wind acceleration in coronal holes. I review the results of
single fluid 2.5D MHD, as well as multi-fluid 2.5D MHD models of waves in coronal holes, the heating, and the acceleration
of the solar wind be these waves. 相似文献
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Examinations of the magnetohydrodynamic (MHD) equations across a bow shock are presented. These equations are written in the familiar Rankine–Hugoniot set, and an exact solution to this set is given which involves the upstream magnetosonic Mach number, plasma , polytropic index, and
B-v
, as a function of position along the shock surface. The asymptotic Mach cone angle of the shock surface is also given as a function of the upstream parameters, as a set of transcendental equations. The standoff position of a detached bow shock from an obstacle is also reviewed. In addition, a detailed examination of the hydrodynamic equations along the boundary of the obstacle is performed. Lastly, the MHD relations along the obstacle surface are examined, for specific orientations of the upstream interplanetary magnetic field (IMF) in relation to the upstream flow velocity vector. 相似文献